Table 2.
Parameters for PSR J1528−3146 from the timing analysis, and derived quantities.
| Observation and data reduction parameters | |
|---|---|
| Span of timing data (MJD) | 52179–59725 |
| Number of TOAs | 13 478 |
| Reference epoch (MJD) | 56 000 |
| Time scale | TCB |
| Solar system ephemeris | DE438 |
| Solar wind electron number density, n0 (cm−3) | 4 |
| Weighted rms residual (μs) | 9.245 |
| Reduced χ2 | 0.993 |
| Astrometric, spin and dispersion parameters | |
| Right ascension, α (J2000) | 15:28:34.95312 (6) |
| Declination, δ (J2000) | −31:46:06.866 (2) |
| Proper motion in α, μα (mas yr−1) | −1.39 (9) |
| Proper motion in δ, μδ (mas yr−1) | −3.7 (2) |
| Spin frequency, ν (Hz) | 16.4413566796379 (11) |
Spin frequency first derivative,  (10−17 Hz s−1) |
−6.7175 (9) |
Spin frequency second derivative,  (10−28 Hz s−2) |
2.8 (6) |
| Dispersion measure, DM (cm−3 pc) | 18.159 (a) |
| Rotation measure, RM (rad m−2) | −19 (1) (b) |
| Binary parameters | |
| Orbital model | DDH |
| Orbital period, Pb (days) | 3.1803502 (2) |
| Projected semi-major axis of the pulsar orbit, x (lt-s) | 11.452301 (11) |
| Epoch of periastron, T0 (MJD) | 56000.7860 (3) |
| Orbital eccentricity, e | 0.0002137 (2) |
| Longitude of periastron, ω (°) | 297.30 (4) |
Rate of advance of periastron,  (° yr−1) |
0.057 (3) |
| Rate of change of orbital semi-major axis, ẋ (10−15 lt-s s−1) | −2.6 (1.9) |
| Orthometric amplitude of the Shapiro delay, h3 (μs) | 1.2 (1) |
| Orthometric ratio of the Shapiro delay, ς | 0.44 (8) |
| Derived parameters | |
| Galactic longitude, l (°) | 337.9386445 |
| Galactic latitude, b (°) | 20.2167420 |
| Total transverse proper motion, μT (mas yr−1) | 3.9 (2) |
| Position angle of proper motion (J2000), Θμ (°) | 200.8 (1.8) |
| DM-derived distance (NE2001), d (kpc) | 0.8(2) (c) |
| DM-derived distance (YWM16), d (kpc) | 0.8(2) (c) |
| Mass function, f (M⊙) | 0.1594451 (5) |
| Spin period, P (ms) | 60.822231369658 (4) |
| Apparent spin period derivative, Ṗ (10−19 s s−1) | 2.4850 (3) |
| Total kinematic contribution to spin period derivative, ΔṖ (10−21 s s−1) | 1.2 (3) (d) |
| Intrinsic spin period derivative (Ṗint) (10−19 s s−1) | 2.473 (3) |
| Spin-down power, Ė (1031 erg s−1) | 4.340 (5) (e) |
| Surface magnetic field strength, Bsurf (109 G) | 3.928 (2) (e) |
| Characteristic age, τc (109 yr) | 3.896 (5) (e) |
| Pulsar mass, Mp (M⊙) |
 (f) |
| Companion mass, Mc (M⊙) |
 (f) |
Notes. Numbers in parentheses are the nominal 1σ statistical uncertainties on the last quoted digits.
DM variations were modeled using piecewise-constant deviations around this value, as enabled by the “DMX” model of Tempo2.
Obtained using the RMcalc program, see Sect. 3 for details.
Distances estimated using the NE2001 (Cordes & Lazio 2002) and YMW16 (Yao et al. 2017) models, assuming a 20% uncertainty.
Contributions from the Shklovskii effect (Shklovskii 1970) and from the differential Galactic acceleration, as calculated using the GalPot model (McMillan 2017; Dehnen & Binney 1998). The uncertainty quoted here corresponds to the maximum excursion from the central value, when varying the pulsar distance by ±20%.
See Lorimer & Kramer (2012) for definitions.
Determined from a Bayesian analysis of the timing data, see Sect. 4.3 for details.
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